Swine Housing With a Belt for Separating Urine and Feces; Key to Flexibility

Kempen, Theo van; Kaspers, Bernd; Burnette, Parren F; Kempen, M. van; Koger, J B

doi:10.13031/2013.15482

Cited by 20 publications

(25 citation statements)

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“…The latter relation was taken as evidence that more massive envelopes have higher accretion rates and thus drive more powerful outflows. van Kempen et al (2010b) speculate that the OH emission originates in the wake of the jet impinging on the dense, inner parts of the envelope, creating dissociative shocks in which [O i] is the dominant coolant, followed by OH (Neufeld & Dalgarno 1989). The relation between OH emission and luminosity supports this scenario.…”

Section: Discussionmentioning

confidence: 83%

“…The expected integrated intensity for HIFI is ∼1.1 K km s −1 for the triplet in total, as calculated from the PACS observation. This value was derived for a 13 beam under the assumption that the source is unresolved, because the OH emission from HH 46 appears to be centrally concentrated (van Kempen et al 2010b). Assuming LTE ratios (∼A ul g u ) for the three components, the strongest transition has an integrated intensity of 0.66 K km s −1 .…”

Section: Discussionmentioning

confidence: 99%

“…In addition, DK Cha and NGC 1333 IRAS 2A were observed with PACS from 55−210 μm at R ∼ 1000 in range spectroscopy mode. Details of the PACS observations of HH 46, NGC 7129 FIRS 2, and DK Cha are described in van Kempen et al (2010b), Fich et al (2010), and van Kempen et al (2010a), respectively. All spectra were reduced with HIPE v2.9.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

“…OH emission at 163.12 μm (1837.8 GHz) was detected with PACS towards the class I YSO HH 46 (van Kempen et al 2010b) …”

Section: Introductionmentioning

confidence: 95%

See 3 more Smart Citations

Herschelobservations of the hydroxyl radical (OH) in young stellar objects

Wampfler¹,

Herczeg

Bruderer³

et al. 2010

A&A

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Section: Discussionmentioning

confidence: 83%

Section: Discussionmentioning

confidence: 99%

Section: Observations and Data Reductionmentioning

confidence: 99%

“…OH emission at 163.12 μm (1837.8 GHz) was detected with PACS towards the class I YSO HH 46 (van Kempen et al 2010b) …”

Section: Introductionmentioning

confidence: 95%

See 2 more Smart Citations

Herschelobservations of the hydroxyl radical (OH) in young stellar objects

Wampfler¹,

Herczeg

Bruderer³

et al. 2010

A&A

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“…The mini-survey by van Kempen et al (2009c) found this narrow extended emission to be ubiquitous in low-mass protostars. Further evidence of UV photon heating was provided by far-infrared CO lines with J u = 10 to 20 observed with Herschel-PACS (van Kempen et al 2010b;Visser et al 2012). However, Herschel has only limited mapping capabilities; PACS lacks velocity resolution and HIFI has a quite large beam (20 -40 ).…”

Section: Introductionmentioning

confidence: 99%

APEX-CHAMP⁺high-JCO observations of low-mass young stellar objects

Yıldız

Kristensen

Dishoeck

et al. 2012

A&A

110

243

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Context. The NGC 1333 IRAS 4A and IRAS 4B sources are among the most well-studied Stage 0 low-mass protostars, which drive prominent bipolar outflows. Spectrally resolved molecular emission lines provide crucial information about the physical and chemical structure of the circumstellar material as well as the dynamics of the different components. Most studies have so far concentrated on the colder parts (T ≤ 30 K) of these regions. Aims. The aim is to characterize the warmer parts of the protostellar envelope using the new generation of submillimeter instruments. This will allow us to quantify the feedback of the protostars on their surroundings in terms of shocks, ultraviolet (UV) heating, photodissociation, and outflow dispersal. Methods. The dual frequency 2 × 7 pixel 650/850 GHz array receiver CHAMP + mounted on APEX was used to obtain a fully sampled, large-scale ∼4 × 4 map at 9 resolution of the IRAS 4A/4B region in the 12 CO J = 6-5 line. Smaller maps were observed in the 13 CO 6-5 and [C i] J = 2-1 lines. In addition, a fully sampled 12 CO J = 3-2 map made with HARP-B on the JCMT is presented and deep isotopolog observations are obtained at selected outflow positions to constrain the optical depth. Complementary Herschel-HIFI and ground-based lines of CO and its isotopologs, from J = 1-0 up to 10-9 (E u /k ≈ 300 K), are collected at the source positions and used to construct velocity-resolved CO ladders and rotational diagrams. Radiative-transfer models of the dust and lines are used to determine the temperatures and masses of the outflowing and photon-heated gas and infer the CO abundance structure. Results. Broad CO emission-line profiles trace entrained shocked gas along the outflow walls, which have an average temperature of ∼100 K. At other positions surrounding the outflow and the protostar, the 6-5 line profiles are narrow indicating UV excitation. The narrow 13 CO 6-5 data directly reveal the UV heated gas distribution for the first time. The amount of UV-photon-heated gas and outflowing gas are quantified from the combined 12 CO and 13 CO 6-5 maps and found to be comparable within a 20 radius around IRAS 4A, which implies that UV photons can affect the gas as much as the outflows. Weak [C I] emission throughout the region indicates that there is a lack of CO dissociating photons. Our modeling of the C 18 O lines demonstrates the necessity of a "drop" abundance profile throughout the envelopes where the CO freezes out and is reloaded back into the gas phase through grain heating, thus providing quantitative evidence of the CO ice evaporation zone around the protostars. The inner abundances are less than the canonical value of CO/H 2 = 2.7 × 10 −4 , however, implying that there is some processing of CO into other species on the grains. The implications of our results for the analysis of spectrally unresolved Herschel data are discussed.

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Belt separation system under slat in fattening pig housing: Effect of belt type and extraction frequency

Alonso

Vázquez

Ovejero

et al. 2010

Bioresource Technology

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The efficiency of manure separation by a conveyor belt under a partially slatted floor for fattening pigs was determined for two types of belts, a fíat belt with an incline of up to 6° transversely and a concave belt with an incline of up to 1° longitudinally. A 31.20% and 23.75% dry matter content of the solid fraction was obtained for the fíat and concave belt, respectively. The fíat belt was more efficient at 6° than other slope angles. The residence time of the manure on the two belt types influenced the separation efficiency from a Uve weight of 63.00 kg upwards. The quantity of residue produced with this system was _ .

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Swine Housing With a Belt for Separating Urine and Feces; Key to Flexibility

Cited by 20 publications

References 0 publications

Herschelobservations of the hydroxyl radical (OH) in young stellar objects

Herschelobservations of the hydroxyl radical (OH) in young stellar objects

APEX-CHAMP⁺high-JCO observations of low-mass young stellar objects

Belt separation system under slat in fattening pig housing: Effect of belt type and extraction frequency

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Swine Housing With a Belt for Separating Urine and Feces; Key to Flexibility

Cited by 20 publications

References 0 publications

Herschelobservations of the hydroxyl radical (OH) in young stellar objects

Herschelobservations of the hydroxyl radical (OH) in young stellar objects

APEX-CHAMP+high-JCO observations of low-mass young stellar objects

Belt separation system under slat in fattening pig housing: Effect of belt type and extraction frequency

Contact Info

Product

Resources

About

APEX-CHAMP⁺high-JCO observations of low-mass young stellar objects